INITIAL CHARACTERISTICS OF KEPLER LONG CADENCE DATA FOR DETECTING TRANSITING PLANETS

By Jon M. Jenkins, Douglas A. Caldwell, H. Chandrasekaran, Joseph D. Twicken, S. Bryson, Elisa Quintana, B. Clarke, Jie Li, C. Allen, P. Tenenbaum and 8 more. 2010

278 citations recorded by the source corpus.

The Kepler Mission seeks to detect Earth-size planets transiting solar-like stars in its ∼115 deg2 field of view over the course of its 3.5 year primary mission by monitoring the brightness of each of ∼156,000 Long Cadence stellar targets with a time resolution of 29.4 minutes. We discuss the photometric precision achieved on timescales relevant to transit detection for data obtained in the 33.5 day long Quarter 1 (Q1) observations that ended 2009 June 15. The lower envelope of the photometric precision obtained at various timescales is consistent with expected random noise sources, indicating that Kepler has the capability to fulfill its mission. The Kepler light curves exhibit high precision over a large dynamic range, which will surely permit their use for a large variety of investigations in addition to finding and characterizing planets. We discuss the temporal characteristics of both the raw flux time series and the systematic error-corrected flux time series produced by the Kepler Science Pipeline, and give examples illustrating Kepler's large dynamic range and the variety of light curves obtained from the Q1 observations.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/586f171c2d5236fd029069fe9cd3c41fe22a0575

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In Astronomy and Astrophysics

1. D. Charbonneau
2. Jon Fortney
3. Timothy Morton
4. J. Winn
5. J. Johnson
6. G. Marcy
7. D. Huber
8. Andrew W. Howard

In Instrumentation

1. D. Charbonneau
2. Timothy Morton
3. Jon Fortney
4. J. Winn
5. J. Southworth
6. J. Johnson
7. D. Huber
8. G. Marcy

Citations in the corpus

• PRE-SPECTROSCOPIC FALSE-POSITIVE ELIMINATION OF KEPLER PLANET CANDIDATES (2010, methodology): “A discussion of the resulting flux timeseries is given in Jenkins et al. (2010b).”
• CHARACTERISTICS OF PLANETARY CANDIDATES OBSERVED BY KEPLER. II. ANALYSIS OF THE FIRST FOUR MONTHS OF DATA (2011, methodology): “Steps such as high-precision RV measurements (Borucki et al. 2010; Koch et al. 2010b; Dunham et al. 2010; Jenkins et al. 2010a; Latham et al. 2010) or transit timing variations (TTVs; Holman et al. 2010; Lissauer et al. 2011a) are used when practical.”
• Rotation and magnetism of Kepler pulsating solar-like stars : Towards asteroseismically calibrated age-rotation relations (2014, methodology): “The magnitude correction of the photon noise from Jenkins et al. (2010) was then applied to the S ph,k.”
• THE APOKASC CATALOG: AN ASTEROSEISMIC AND SPECTROSCOPIC JOINT SURVEY OF TARGETS IN THE KEPLER FIELDS (2014, methodology): “Preparation of Kepler long-cadence data (Jenkins et al. 2010) for asteroseismic analysis was handled in three cohorts.”
• OVERVIEW OF THE KEPLER SCIENCE PROCESSING PIPELINE (2010, background): “In spite of the presence of these image artifacts, Kepler is already achieving photometric precision sufficient to detect Earth-size planets transiting solar-like stars for the majority of the FOV at any given time (Jenkins et al. 2010).”
• KEPLER ECLIPSING BINARY STARS. II. 2165 ECLIPSING BINARIES IN THE SECOND DATA RELEASE (2011, methodology): “124 additional systems were identified as EBs in the Q2 data from the Kepler Transit Planet Search (TPS) output.”
• AN ANCIENT EXTRASOLAR SYSTEM WITH FIVE SUB-EARTH-SIZE PLANETS (2015, methodology): “We investigated the planetary and orbital properties of the Kepler-444 system using long- cadence Kepler data (∆t ∼ 30 min; Jenkins et al. 2010).”
• ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS (2010, methodology): “Firstly, in some cases data from different quarters show intensity discontinuities that are mainly caused by pixel shifts after reorientation of the spacecraft (Jenkins et al. 2010).”
• Homogeneous studies of transiting extrasolar planets – IV. Thirty systems with space-based light curves (2011, background): “The third light value given by Jenkins et al. (2010a) does not have an errorbar, so Iad pt L3 = 0.0075±0.0075 to be conservative.”
• KEPLER-18b, c, AND d: A SYSTEM OF THREE PLANETS CONFIRMED BY TRANSIT TIMING VARIATIONS, LIGHT CURVE VALIDATION, WARM-SPITZER PHOTOMETRY, AND RADIAL VELOCITY MEASUREMENTS (2011, methodology): “The data from the spacecraft are processed through the Kepler Science Operations Center pipeline (Jenkins et al. 2010c) to perform standard CCD processing and to remove instrumental artifacts.”
• LACK OF INFLATED RADII FOR KEPLER GIANT PLANET CANDIDATES RECEIVING MODEST STELLAR IRRADIATION (2011, methodology): “Method For each of the 115 KOI, we retrieved the Q0-Q2 raw long-cadence photometry (Jenkins et al. 2010) from MAST2.”
• KEPLER ECLIPSING BINARY STARS. I. CATALOG AND PRINCIPAL CHARACTERIZATION OF 1879 ECLIPSING BINARIES IN THE FIRST DATA RELEASE (2010, methodology): “…is a wavelet-based, adaptive matched filter that characterizes the power spectral density (PSD) of the background process that yields the observed light curve and uses this time-variable PSD estimate to realize a pre-whitening filter and whiten the light curve (Jenkins 2002; Jenkins et al. 2010d).”
• KEPLER MISSION STELLAR AND INSTRUMENT NOISE PROPERTIES (2011, methodology): “To give the full CDPP, we added (in variance space) a contribution to represent shot noise which was calibrated on a linear interpolation (random on [0,1] by star) of the minimal LC noise and upper envelope noise models presented in Jenkins et al. (2010b).”
• PHOTOMETRIC VARIABILITY IN KEPLER TARGET STARS. II. AN OVERVIEW OF AMPLITUDE, PERIODICITY, AND ROTATION IN FIRST QUARTER DATA (2010, methodology): “We use only the so-called Long Cadence data which is formed on-board the spacecraft by summing 270 6 second integrations into successive 29.42 minute blocks (see (Jenkins et al. 2010a) for additional details).”
• Kepler Presearch Data Conditioning I—Architecture and Algorithms for Error Correction in Kepler Light Curves (2012, methodology): “The vast majority of these discontinuities are the result of cosmic rays or solar energetic particles striking the photometer and causing permanent local changes in pixel sensitivity, although partial exponential recovery is often observed (Jenkins et al. 2010b).”
• Asteroseismology of old open clusters with Kepler: direct estimate of the integrated red giant branch mass-loss in NGC 6791 and 6819 (2011, methodology): “The data reduction from raw images to the final light curves is described by Jenkins et al. (2010a), Garćıa et al. (2011), and Stello et al. (2011a).”
• PLANET HUNTERS: A TRANSITING CIRCUMBINARY PLANET IN A QUADRUPLE STAR SYSTEM (2012, background): “The Transiting Planet Search (TPS) (Tenenbaum et al. 2012; Jenkins et al. 2010b, 2002) pipeline and the candidate vetting process were primarily designed to identify transiting planets around single stars (Batalha et al. 2013).”